Structure Scalars in Charged Plane Symmetry

Sharif, M.; Bhatti, M. Z.

doi:10.1142/s0217732312501416

Cited by 61 publications

(31 citation statements)

References 24 publications

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“…Thus the trace-free part of the tensor, X αβ , does have some significance in the structure and evolution of self-gravitating stars. Equation (48) indicates that if μ = μ(z), then X T F = 0 and vice versa, thereby representing X T F as a parameter of controlling the irregularities in anisotropic stellar systems, which supports the analysis of [41], [43][44][45][46][47][48]. Moreover, the gravitational contribution due to Palatini f (R) terms does not disrupt the significance of the modified structure scalars X T F .…”

Section: Anisotropic Fluidsupporting

confidence: 58%

“…Furthermore, Herrera et al [43] explored the consequences of the cosmological constant for radiating spherical relativistic collapse by evaluating the shear and expansion evolution equations. Sharif and Bhatti [44,45] extended their results for planar and cylindrical compact objects. Herrera [46] investigated the causes of density irregularities in radiating spherical stellar systems and explored some inhomogeneity factors.…”

Section: Introductionmentioning

confidence: 83%

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Stability of regular energy density in Palatini $$f(R)$$ f ( R ) gravity

Sharif

Yousaf

2015

Eur. Phys. J. C

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The present work explores the effects of the three-parametric f (R) model on the stability of the regular energy density of planar fluid configurations with the Palatini f (R) formalism. For this purpose, we develop a link between the Weyl scalar and structural properties of the system by evaluating a couple of differential equations. We also see the effects of Palatini f (R) terms in the formulation of structure scalars obtained by orthogonal splitting of the Riemann tensor in general relativity. We then identify the parameters which produce energy density irregularities in expansive and expansion-free dissipative as well as non-dissipative matter distributions. It is found that particular combinations of the matter variables lead to irregularities in an initially homogeneous fluid distribution. We conclude that Palatini f (R) extra corrections tend to decrease the inhomogeneity, thereby imparting stability to the self-gravitating system.

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Section: Anisotropic Fluidsupporting

confidence: 58%

Section: Introductionmentioning

confidence: 83%

Stability of regular energy density in Palatini $$f(R)$$ f ( R ) gravity

Sharif

Yousaf

2015

Eur. Phys. J. C

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“…The effects of electromagnetic field on structure scalars and dynamics of self-gravitating objects have been explored by Herrera and his collaborators (Herrera et al 2011, Diprisco et al 2007). Sharif and his collaborators (Sharif and Bhatti 2012a, Sharif and Bhatti 2012b, Sharif and Bhatti 2013a, Sharif and Bhatti 2013b, Sharif and Bhatti 2014, Sharif and Yousaf 2012, Sharif and Kausar 2011 have extended this work for cylindrical and plane symmetries in GR as well as in f (R) gravity with electromagnetic field. This paper is organized as follows: In section 2, charged anisotropic cylindrical source and Einstein-Maxwell equations have presented.…”

Section: Introductionmentioning

confidence: 96%

Gravitational collapse and expansion of charged anisotropic cylindrical source

Mahmood

Shah

Abbas

2015

Astrophys Space Sci

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In this paper, we have discussed the gravitational collapse and expansion of charged anisotropic cylindrically symmetric gravitating source. To this end, the generating solutions of Einstein-Maxwell field equations for the given source and geometry have been evaluated. We found the auxiliary solution of the filed equations, this solution involves a single function which generates two kinds of anisotropic solutions. Every solution can be expressed in terms of arbitrary function of time that has been chosen arbitrarily to fit the various astrophysical time profiles. The existing solutions predict gravitational collapse and expansion depending on the choice of initial data. Instead of base to base collapse, in the present case, wall to wall collapse of the cylindrical source has been investigated. We have found that the electromagnetic field is responsible for the enhancement of anisotropy in collapsing system.

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“…A lot of discussion about the complexity has been assessed in various fields of science. Now in this attention several researchers have given systematic work that is shown in [1][2][3][4][5][6][7][8][9][10].…”

Section: Introductionmentioning

confidence: 99%

Complexity factor for static anisotropic self-gravitating source in f(R) gravity

Abbas

Nazar

2018

Eur. Phys. J. C

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In a recent paper, Herrera (Phys Rev D 97: 044010, 2018) have proposed a new definition of complexity for static self-gravitating fluid in general relativity. In the present article, we implement this definition of complexity for static self-gravitating fluid to case of f (R) gravity. Here, we found that in the frame of f (R) gravity the definition of complexity proposed by Herrera, entirely based on the quantity known as complexity factor which appears in the orthogonal splitting of the curvature tensor. It has been observed that fluid spheres possessing homogenous energy density profile and isotropic pressure are capable to diminish their the complexity factor. We are interested to see the effects of f (R) term on complexity factor of the self-gravitating object. The gravitating source with inhomogeneous energy density and anisotropic pressure have maximum value of complexity. Further, such fluids may have zero complexity factor if the effects of inhomogeneity in energy density and anisotropic pressure cancel the effects of each other in the presence of f (R) dark source term. Also, we have found some interior exact solutions of modified f (R) field equations satisfying complexity criterium and some applications of this newly concept to the study of structure of compact objects are discussed in detail. It is interesting to note that previous results about the complexity for static self-gravitating fluid in general relativity can be recovered from our analysis if f (R) = R, which general relativistic limit of f (R) gravity.

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Structure Scalars in Charged Plane Symmetry

Cited by 61 publications

References 24 publications

Stability of regular energy density in Palatini $$f(R)$$ f ( R ) gravity

Stability of regular energy density in Palatini $$f(R)$$ f ( R ) gravity

Gravitational collapse and expansion of charged anisotropic cylindrical source

Complexity factor for static anisotropic self-gravitating source in f(R) gravity

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